We aim to establish and improve the accuracy level of asteroseismic estimates of mass , radius , and age of giant stars .
This can be achieved by measuring independent , accurate , and precise masses , radii , effective temperatures and metallicities of long period eclipsing binary stars with a red giant component that displays solar-like oscillations .
We measured precise properties of the three eclipsing binary systems KIC 7037405 , KIC 9540226 , and KIC 9970396 and estimated their ages be 5.3 \pm 0.5 , 3.1 \pm 0.6 , and 4.8 \pm 0.5 Gyr .
The measurements of the giant stars were compared to corresponding measurements of mass , radius , and age using asteroseismic scaling relations and grid modeling .
We found that asteroseismic scaling relations without corrections to \Delta \nu systematically overestimate the masses of the three red giants by 11.7 % , 13.7 % , and 18.9 % , respectively .
However , by applying theoretical correction factors f _ { \Delta \nu } according to \citet Rodrigues2017 , we reached general agreement between dynamical and asteroseismic mass estimates , and no indications of systematic differences at the precision level of the asteroseismic measurements .
The larger sample investigated by \citet Gaulme2016 showed a much more complicated situation , where some stars show agreement between the dynamical and corrected asteroseismic measures while others suggest significant overestimates of the asteroseismic measures .
We found no simple explanation for this , but indications of several potential problems , some theoretical , others observational .
Therefore , an extension of the present precision study to a larger sample of eclipsing systems is crucial for establishing and improving the accuracy of asteroseismology of giant stars .